Some Effects of Earthquakes, Temperature, Wind Stor ms and Barometric Pressure on the Inter ferometer at Hanford Robert Schofield Masahiro Ito Rauha Rahkola Evan Mauceli Ray Frey David Strom Jim Brau University of Oregon Some Concerns With Low Frequency Influences · Loss of lock · Need for increased servo loop gain · May eat up actuator range · Possible increased background in the LIGO frequency band · Possible modulation of noise in the LIGO band Guralp ...

... Orion Star Colours . ... Red stars are cool, around 3,000 kelvins (K), while blue stars are hotter and can have temperatures over 30,000 K. Our own lovely yellow Sun's temperature is a comforting 6,000 K. Hydrogen Trifid . ... Clouds of glowing hydrogen gas mingle with dark dust lanes in the Trifid Nebula, a star forming region in the constellation Sagittarius. ... These are galaxies of the Hercules Cluster, an archipelago of "island universes" a mere 650 million light-years distant. ... Vega . ...

... This loss depends on several parameters, in particular on the position where the photon was detected, its energy, the temperature of the CCD, and the saturation of traps by charges preceding along the readout direction. ... For deriving the CTI, each CCD column was split into macro pixels, which were determined by adaptive binning to contain a sufficient number of first singles around the line feature. ...

Blackholes2 Forum Message . ... Holostars: Black Holes Without Event Horizons . ... Its name derives from the fact tht information is preserved in such a black hole, and must be a contraction of hologram and star. ... The exterior metrics and fields of the charged holostar are equal to the Reissner-Nordstroem black hole solution. ... www.astronomy.net . ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... GSAOI Home . ... Science . ... Despite vast increase in our understanding of the evolutionary nature of planetary nebulae (PNe) during the last three decades, a central question remains: where is the missing mass? Theoretical evolutionary tracks predict that all stars with masses in the range 1.4-8 M Sun should become PNe. ... Clearly, much of the mass of the planetary nebula shell must remain un-ionized, and much of it may be in molecular form. ... The Magellanic Cloud PNe are ideal for this. ...

PROTOCOL OF THE INTERNATIONAL MEETING ON "WARNING" MISSION . ... According to the National Space Program of Ukraine on 1998-2002 the experimental space system WARNING has to be designed and launched in 2001. ... Composition of scientific payload is implemented in the international cooperation. ... Lviv Center of Space Research Institute (LC SRC), Ukraine. ... Space Research Institute NASU-NSAU (SRI), Kiev, UKRAINE; . ... Lviv Center of Space Research Institute (LC SRI), Lviv, UKRAINE; . ...

Lunar and Planetary Science XXXIV (2003) 1575.pdf MAJOR AND TRACE ELEMENT CHEMISTRY AND Ar-Ar AGE OF THE NWA E.V. Korotchantseva1,2, M.A. Ivanova1, C.A. Lorenz1, A.I. Bouikine1,2, M. Trieloff2, Promprated3, M. Anand3, and L.A. Taylor3 : ... Universitфt Heidelberg, Germany; 3Planetary Geosciences Institute, University of Tennessee, Knoxville, T Introduction: Northwest Africa ( NWA ) 011 was originally described as a non-cumulate eucrite with an anomalous Fe/Mn ratio [1] ... REEs of NWA 011. ...

... Space Contents 1-2 YEAR 3-4 MONTH 5-6 DAY 7-8 BLANK 9-12 N (THE NORTHERN HEMISPHERE aa DAILY VALUE ) 13-15 BLANK 16-19 S (THE SOUTHERN HEMISPHERE aa DAILY VALUE ) 20-22 BLANK 23-26 M1 (HALF DAILY VALUE OF aa INDICES FOR THE GREENWICH DAY ) 27-29 BLANK 30-33 M2 (SECOND HALF DAILY VALUE OF aa INDICES FOR GREENWICH DAY ) 34-36 BLANK 37-38 CC_OR_K (QUIET DAYS CLASSIFICATION) 39-41 MONTHLY MEAN DATA: Loacated after the last day of the month. ...

... Determination of the Permissible Solutions Area by Image Reconstruction from a few Projections: Method 2­CLEAN DSA Michail I. Agafonov Radiophysical Research Institute (NIRFI), 25 B.Pecherskaya st., Nizhny Novgorod, 603600, Russia, E­mail: agfn@nirfi.nnov.su Abstract. ... Application The problem requires the solution of the equation G = H # F (+noise) , (1) where F (x, y) is the object brightness distribution, H(x, y) is the fan (dirty) beam, and G(x, y) is the dirty (summary) image. ...

... All rights reserved Printed in Great Britain 0273-l 177/00 $20.00 + 0.00 PII: SO273-1177(99)01221-I ELECTRIC FIELD DISTURBANCE IN THE EARTH - IONOSPHERE LAYER V. M. Sorokin , and A. K. Yaschenko Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS (IZMlRAN), Troitsk, Moscow region, 142092, Russia ABSTRACT Theoretical studies of the electric field disturbance due to a variation of the atmospheric current, flowing between ionosphere and the Earth, are carried out. ...

Instruments and Methods 133 Sky temperature resolution by microwave radiometry A.G. Kislyakov State University, Nizhny Novgorod, Russia Introduction The threshold sensitivity of a radiometer is determined by well known equation Karlov & Manenkov, 1966 " hE i = h hn i +1 hn i + N t G0 , 1 G0 1=2 : 1 Here we denote hE ias the minimum detectable increment of radiation spectral density E at a frequency . ... Equation 3 gives a correction to the expression for limit detector sensitivity Kislyakov, 1997. ...

... For more distant stars we must use other techniques. ... Hence if we see a distant galaxy and can pick out any cepheids lying within it, we can calculate its distance. ... Here then is another method to gauge the size of the Universe and there are yet more. volume at high enough temperature a nuclear fusion reaction sweeps across the white dwarf's surface and eventually we will see a spectacularly bright new star (hence nova) in our skies. ... Why is this relevant to the size of the Universe? ...

Detection technique . We are using ISIS , the optimal image subtraction method developed by C. Alard & R.H. Lupton, to search for SNe in our images. ... The second image shows the same subtraction, but after the convolution of the best image with ISIS: . ... For this reason, we are suggested to search for nuclear SNe with NICMOS on HST, to exploit its stable PSF, sensitivity and angular resolution to detect from space nuclear obscured SNe which might have been missed by ground-based surveys. ...

Ralph: Visible and infrared imager/spectrometer; provides color, composition and thermal maps. Alice: Ultraviolet imaging spectrometer; analyzes composition and structure of Pluto's atmosphere and looks for atmospheres around Charon and Kuiper Belt objects (KBOs). REX: Measures atmospheric composition and temperature; passive radiometer. ... SWAP: Solar wind and plasma spectrometer; measures atmospheric "escape rate" and observes Pluto's interaction with solar wind. ...

spaceweb@oulu.fi - last update: 11 May 1998, 0900 UT . Matter in the known universe can be classified in terms of four states: solid, liquid, gaseous, and plasma . The basic distinction between solids, liquids and gases lies in the difference between the strength of the bonds that hold their constituent particles together. ... On the other hand, the transition from a gas to an ionized gas, i.e., plasma , is not a phase transition, since it occurs gradually with increasing temperature. ...

... We had a unique diagnostic tool for determining whether or not the secondary was fractured during the dark run in that we had 3 sets of focus sweep data for the imaging camera taken on the nights of 05 October 1999, 11 October 1999, and 14 October 1999. ... Figure: 05 October 1999, CCD g1 . ... Surface plot. ... Figure 32 plots the same data but for CCD g3. ... Figure: Comparison of normalised brighness for the out-of-focus doughnuts for the nights of 05, 11, and 14 October 1999 for CCD g1. ...

... 2011 February 11 . Star Colors in Orion . ... Explanation: What determines a star's color ? ... Red stars are cool, with surface temperatures of around 3,000 kelvins (K) , while blue stars are hotter and can have temperatures over 30,000 K. Our own lovely "yellow" Sun's temperature is a comforting 6,000 K. Differences in star colors are particularly easy to see in this intriguing composite view of the constellation Orion, made while experimenting with a star trail step-focus technique . ...

This test was is performed to investigate the feasibility of CMOS amplifiers (TLC 27481) at cryogenic temperatures for use with InSb FPA's. The advantage of cryogenic amplifiers is the possibility to place them close to the FPA. The video signal is amplified directly at the detector. ... If the cryogenic amplifier is switched on the temperature of the detector board is increased from 100 K to 125 K (third curve from bottom in figure 1 ). ... Third curve from bottom: temperature of detector board. ...

... Dept. for Physics of Stars&Galaxies . ... Using a database view Sloan Digital Sky Survey (SDSS), containing almost a million spectra created 15,000 sample galaxies with active star formation, which is used for various studies and physical state of evolution of galaxies. ... Star clusters of the Galaxy . The project MWSC (Milky Way Star Clusters) directory using 2MASS, which includes nearly 500 million vision to the limit Ks = 15.3, analyzed more than 4,000 cluster-like objects in the galaxy. ...

... 18941904; Bespalov P.A. Effective saturation of absorption in a plasma magnetospheric maser. In book: Nonlinear Space Plasma Physics, R.Z. Sagdeev -Editor-in-Chief, American Institute of Physics, 1993, p.339-346]. Magnetospheric plasma maser [Bespalov P.A, Trakhtengerts V.Yu., ... In a magnetospheric plasma maser (MPM) the relatively dense magnetised plasma and the conjugate ends of a magnetic trap form a quasioptical resonator for electromagnetic waves. ...